15th HEAD Naples, FL – April, 2016 Meeting Program Session Table of Contents 100 – AGN I Analysis Poster Session 206 – Early Results from the Astro-H 101 – Galaxy Clusters 116 – Missions & Instruments Poster Mission 102 – Dissertation Prize Talk: Accretion Session 207 – Stellar Compact II driven outflows across the black hole mass 117 – Solar and Stellar Poster Session 300 – The Physics of Accretion Disks – A scale, Ashley King (KIPAC/Stanford 118 – Supernovae and Supernova Joint HEAD/LAD Session University) Remnants Poster Session 301 – Gravitational Waves 103 – Time Domain Astronomy 119 – WDs & CVs Poster Session 302 – Missions & Instruments 104 – Feedback from Accreting Binaries in 120 – XRBs and Population Surveys Poster 303 – Mid-Career Prize Talk: In the Ring Cosmological Scales Session with Circinus X-1: A Three-Round Struggle 105 – Stellar Compact I 200 – Solar Wind Charge Exchange: to Reveal its Secrets, Sebastian Heinz 106 – AGNs Poster Session Measurements and Models (Univ. of Wisconsin) 107 – Astroparticles, Cosmic Rays, and 201 – TeraGauss, Gigatons, and 304 – Science of X-ray Polarimetry in the Neutrinos Poster Session MegaKelvin: Theory and Observations of 21st Century 108 – Cosmic Backgrounds and Deep Accretion Column Physics 305 – Making the Multimessenger – EM Surveys Poster Session 202 – The Structure of the Inner Accretion Connection 109 – Galactic Black Holes Poster Session Flow of Stellar-Mass and Supermassive 306 – SNR/GRB/Gravitational Waves 110 – Galaxies and ISM Poster Session Black Holes 400 – AGN II 111 – Galaxy Clusters Poster Session 203 – Missing Baryons and the Hot Halo of 401 – The Unique Role of Very High 112 – Gamma-Ray Bursts Poster Session the Milky Way Energy Observations in Multi-Wavelength 113 – Gravitational Waves Poster Session 205 – Plenary Talk: Observation of Astronomy 114 – Isolated Nss Poster Session Gravitational Waves in Advanced LIGO, 402 – Dark Matter, ISM, & Galaxies 115 – Laboratory Astrophysics and Data Laura Cadonati (Georgia Tech) 403 – Rapporteur Plenary Talk imaging and polarimetry can give us clues to the locations of the 100 – AGN I radiating particles in each band, as well as their kinematics and the jet's structure. We discuss new work that describes how 100.01 – An HST proper-motion study of the optical observations in several bands can be knit together to form a more jet in 3C 264: Direct Evidence for the Internal Shock coherent picture of jet physics. Model Some of the most energetic phenomena in the Universe involve Author(s): Eric S. Perlman1, Sayali S Avachat1 , Devon highly relativistic flows, in which particles are accelerated up to TeV Clautice1332 , Markos Georganopoulos , Eileen Meyer , Mihai Cara energies. In the case of relativistic jets from Active Galactic Nuclei Institution(s): 1. Florida Institute of Technology, 2. Space (AGN), these flows can carry enough energy to significantly Telescope Science Institute, 3. UMBC influence both galactic and cluster evolution. While the exact physical mechanism that accelerates the radiating particles within 100.03 – New insights into AGN coronae the jet is not known, a widely adopted framework is the internal Active galactic nuclei (AGN) are some of the most energetic sources shock model, invoked to explain high-energy, non-thermal of radiation in the Universe. The conversion of gravitational energy radiation from objects as diverse as microquasars, gamma-ray into radiation is thought to take place in an accretion disk/corona bursts, and relativistic jets in AGN. This model posits an unsteady system just outside the black hole. In this system thermal, relativistic flow that gives rise to components in the jet with UV/optical photons from the accretion disk are upscattered in a different speeds. Faster components catch up to and collide with corona of hot electrons situated above the accretion disk producing slower ones, leading to internal shocks. Despite its wide popularity X-rays. The nature of this Comptonizing corona remains a key as a theoretical framework, however, no occurance of this open question in AGN physics. The NuSTAR satellite provides the mechanism has ever been directly observed. We will present opportunity to study the Comptonization spectrum produced by evidence of such a collision in a relativistic jet observed with the the corona in great detail. In our talk we will show some key results Hubble Space Telescope (HST) in the nearby radio galaxy 3C 264 from these new studies of the Comptonization spectrum. We (Meyer et al., 2015, Nature). Using images taken over 20 years, we explore how, together with our growing knowledge of coronal sizes, show that a bright ‘knot’ in the jet is moving at an apparent speed of we are able to draw first conclusions about the physics taking place 7.0 +/- 0.8c and is in the incipient stages of a collision with a in the corona. We find evidence for coronae to be hot and slow-moving knot (1.8 +/- 0.5c) just downstream. In the most radiatively compact, putting them close to the boundary of the recent epoch of imaging, we see evidence of brightening of the two region in the compactness–temperature diagram which is knots as they commence their kiloparsec-scale collision. This is the forbidden due to runaway pair production. This suggests that pair behaviour expected in the internal shock scenario and the first production and annihilation are essential ingredients in the direct evidence that internal shocks are a valid description of coronae of AGN and that they control the coronal temperature and particle acceleration in relativistic jets. shape of the observed spectra. Author(s): Eileen T. Meyer4, Markos Georganopoulos4 , Author(s): Anne Lohfink2, Andrew C Fabian21 , Julien Malzac , William B. Sparks31 , Eric S. Perlman , Roeland P. Van Der Marel 3 , Renaud Belmont12 , Douglas Buisson Jay Anderson32 , S. Tony Sohn , John A. Biretta 3 , Colin Arthur Institution(s): 1. Universite de Toulouse, 2. University of Norman23 , Marco Chiaberge Cambridge Institution(s): 1. Florida Institute of Technology, 2. Johns Hopkins University, 3. Space Telescope Science Institute, 4. 100.04 – Chandra solves the mystery: Understanding University of Maryland, Baltimore County the UV anomaly discovered by HST A strange anomaly was discovered during our 180 day HST 100.02 – Multiwavelength Observations of AGN Jets: campaign to observe NGC5548 for reverberation mapping. The UV Untangling the Coupled Problems of Emission emission lines responded to changes in the UV continuum, as they Mechanism and Jet Structure should, during most of The discovery of X-ray and optical emission from large numbers of the observing season. However, there was a period of about 60--70 AGN jets is one of the key legacies of the Chandra X-ray days during which the UV emission lines decorrelated from Observatory and Hubble Space Telescope. Several dozen optical continuum variations. Understanding this anomaly is vital to the and X-ray emitting jets are now known, most of which are seen in success of reverberation mapping technique. We also observed the both bands as well as in the radio, where they were first discovered. source 4 times with Chandra during the 180 day HST observations. Jets carry prodigious amounts of energy and mass out from the Chandra observations revealed the presence of soft excess during nuclear regions out to tens to hundreds of kiloparsecs distant from the anomaly, but there was no soft excess before or after the the central black hole, depositing it into the host galaxy and cluster. anomaly. This suggests that the accretion disk temperature Interpreting their multiwavelength emissions has not been easy: increased from the ``normal'' state, peaking in FUV, to that while in most jets, the optical and radio emission in many objects is peaking in soft X-rays during the anomaly. Thus, there was no believed to emerge via the synchrotron process, due to its ionizing continuum to which to reverberate. There are more characteristic spectral shape and high radio polarization, the X-ray curious things about the response of emission lines, such as the emission has been a tougher nut to crack. In less powerful, FR I time at which the anomaly sets in and the amount flux decrease jets, such as M87, the X-ray emission is believed to be synchrotron during the anomaly. I will discuss the details of this first-of-its-kind emission from the highest energy electrons, requiring in situ behavior and present detailed explanation. particle acceleration due to the short radiative lifetimes of the particles. However, in FR II and quasar jets, a variety of emission Author(s): Smita Mathur1, Anjali Gupta1 mechanisms are possible. Until the last few years, the leading Institution(s): 1. The Ohio State University interpretation had been inverse-Comptonization of Cosmic Microwave Background photons (the IC/CMB mechanism). This 100.05 – A New Look at Ionized Disk Winds in requires the jet to be relativistic out to hundreds of kiloparsecs Seyfert-1 AGN from the nucleus, and requires an electron spectrum that extends to very low Lorentz factors. However, that now appears less likely, We present an analysis of deep, high signal-to-noise due to observed high optical polarizations in jets where the optical Chandra/HETG observations of four Seyfert-1 galaxies with known and X-ray emission appears to lie on the same spectral component, warm absorbers (outflowing winds), including NGC 4151, as well as limits derived from Fermi observations in the GeV MCG-6-30-15, NGC 3783, and NGC 3516. Focusing on the 4-10 gamma-rays. It now appears more likely that the X-rays must arise keV Fe K-band, we fit the spectra using grids of models as synchrotron emission from a second, high energy electron characterized by photoion- ized absorption. Even in this limited population. With this revelation, we must tackle anew the coupling band, the sensitive, time-averaged spectra all require 2-3 zones between jet structure and emission mechanisms.